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The Einstein Telescope: a Third-Generation Gravitational Wave Observatory Home Search Collections Journals About Contact us My IOPscience The Einstein Telescope: a third-generation gravitational wave observatory This article has been downloaded from IOPscience. Please scroll down to see the full text article. 2010 Class. Quantum Grav. 27 194002 (http://iopscience.iop.org/0264-9381/27/19/194002) View the table of contents for this issue, or go to the journal homepage for more Download details: IP Address: 194.94.224.254 The article was downloaded on 18/02/2013 at 07:48 Please note that terms and conditions apply. IOP PUBLISHING CLASSICAL AND QUANTUM GRAVITY Class. Quantum Grav. 27 (2010) 194002 (12pp) doi:10.1088/0264-9381/27/19/194002 The Einstein Telescope: a third-generation gravitational wave observatory M Punturo1,2, M Abernathy3, F Acernese4,5, B Allen6, N Andersson7, K Arun8, F Barone4,5, B Barr3, M Barsuglia9,MBeker10, N Beveridge3, S Birindelli11,SBose12,LBosi1, S Braccini13, C Bradaschia13, T Bulik14, E Calloni4,15, G Cella13, E Chassande Mottin9, S Chelkowski16, A Chincarini17, J Clark18, E Coccia19,20, C Colacino13,JColas2, A Cumming3, L Cunningham3, E Cuoco2, S Danilishin21, K Danzmann6, G De Luca22, R De Salvo23, T Dent18, R De Rosa4,15,LDiFiore4,15, A Di Virgilio13, M Doets10, V Fafone19,20, P Falferi24, R Flaminio25, J Franc25, F Frasconi13,AFreise16,PFulda16,JGair26, G Gemme17, A Gennai16, A Giazotto2,13, K Glampedakis27, M Granata9,HGrote6, G Guidi28,29, G Hammond3, M Hannam30, J Harms31, D Heinert32, M Hendry3, I Heng3, E Hennes10, S Hild3, J Hough4,SHusa33, S Huttner3, G Jones18, F Khalili21, K Kokeyama16, K Kokkotas27, B Krishnan33, M Lorenzini28,HLuck¨ 6, E Majorana34, I Mandel35,36, V Mandic31, I Martin3, C Michel25, Y Minenkov19,20, N Morgado25, S Mosca4,15, B Mours37,HMuller–Ebhardt¨ 6, P Murray3, R Nawrodt3, JNelson3, R Oshaughnessy38,CDOtt39,CPalomba34, A Paoli2, G Parguez2, A Pasqualetti2, R Passaquieti13,40, D Passuello13, L Pinard25, R Poggiani13,40, P Popolizio2, M Prato17, P Puppo34, D Rabeling10, P Rapagnani34,41, J Read33, T Regimbau11, H Rehbein6, SReid3, L Rezzolla33, F Ricci34,41, F Richard2, A Rocchi19, S Rowan3, ARudiger¨ 6, B Sassolas25, B Sathyaprakash18, R Schnabel6, C Schwarz42, P Seidel42, A Sintes33, K Somiya39, F Speirits3, K Strain3, S Strigin21, P Sutton18, S Tarabrin21,AThuring¨ 6, J van den Brand10, C van Leewen10, M van Veggel3, C van den Broeck18, A Vecchio16, JVeitch16, F Vetrano28,29, A Vicere28,29, S Vyatchanin21, B Willke6, G Woan3, P Wolfango43 and K Yamamoto6 1 INFN, Sezione di Perugia, I-6123 Perugia, Italy 2 European Gravitational Observatory (EGO), I-56021 Cascina (Pi), Italy 3 Department of Physics and Astronomy, The University of Glasgow, Glasgow, G12 8QQ, UK 4 INFN, Sezione di Napoli, Italy 5 Universita` di Salerno, Fisciano, I-84084 Salerno, Italy 6 Max-Planck-Institut fur¨ Gravitationsphysik, D-30167 Hannover, Germany 7 University of Southampton, Southampton SO17 1BJ, UK 8 LAL, Universite´ Paris-Sud, IN2P3/CNRS, F-91898 Orsay, France 9 AstroParticule et Cosmologie (APC), CNRS; Observatoire de Paris-Universite´ Denis Diderot-Paris VII, France 10 VU University Amsterdam, De Boelelaan 1081, 1081 HV, Amsterdam, The Netherlands 11 Universite´ Nice ‘Sophia-Antipolis’, CNRS, Observatoire de la Coteˆ d’Azur, F-06304 Nice, France 12 Washington State University, Pullman, WA 99164, USA 13 INFN, Sezione di Pisa, Italy 0264-9381/10/194002+12$30.00 © 2010 IOP Publishing Ltd Printed in the UK & the USA 1 Class. Quantum Grav. 27 (2010) 194002 M Punturo et al 14 Astro. Obs. Warsaw Univ. 00-478; CAMK-PAM 00-716 Warsaw; Bialystok Univ. 15-424; IPJ 05-400 Swierk–Otwock; Inst. of Astronomy 65-265 Zielona Gora, Poland 15 Universita` di Napoli ‘Federico II’, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy 16 University of Birmingham, Birmingham, B15 2TT, UK 17 INFN, Sezione di Genova, I-16146 Genova, Italy 18 Cardiff University, Cardiff, CF24 3AA, UK 19 INFN, Sezione di Roma Tor Vergata I-00133 Roma, Italy 20 Universita` di Roma Tor Vergata, I-00133, Roma, Italy 21 Moscow State University, Moscow, 119992, Russia 22 INFN, Laboratori Nazionali del Gran Sasso, Assergi l’Aquila, Italy 23 LIGO, California Institute of Technology, Pasadena, CA 91125, USA 24 INFN, Gruppo Collegato di Trento, Sezione di Padova; Istituto di Fotonica e Nanotecnologie, CNR-Fondazione Bruno Kessler, 38123 Povo, Trento, Italy 25 Laboratoire des Materiaux´ Avances´ (LMA), IN2P3/CNRS, F-69622 Villeurbanne, Lyon, France 26 University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK 27 Theoretical Astrophysics (TAT) Eberhard-Karls-Universitat¨ Tubingen,¨ Auf der Morgenstelle 10, D-72076 Tubingen,¨ Germany 28 INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Italy 29 Universita` degli Studi di Urbino ‘Carlo Bo’, I-61029 Urbino, Italy 30 Department of Physics, University of Vienna, Boltzmanngasse 5, A-1090 Vienna, Austria 31 University of Minnesota, Minneapolis, MN 55455, USA 32 Friedrich-Schiller-Universitat¨ Jena PF 07737 Jena, Germany 33 Max Planck Institute for Gravitational Physics (Albert Einstein Institute) Am Muhlenberg¨ 1, D-14476 Potsdam, Germany 34 INFN, Sezione di Roma 1, I-00185 Roma, Italy 35 Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA 36 NSF Astronomy and Astrophysics Postdoctoral Fellow 37 LAPP-IN2P3/CNRS, Universite´ de Savoie, F-74941 Annecy-le-Vieux, France 38 The Pennsylvania State University, University Park, PA 16802, USA 39 Caltech–CaRT, Pasadena, CA 91125, USA 40 Universita` di Pisa, I-56127 Pisa, Italy 41 Universita` ‘La Sapienza’, I-00185 Roma, Italy 42 INFN, Sezione di Roma Tre and Universita` di Roma Tre—Dipartimento di Fisica, I-00146 Roma, Italy 43 Universita` degli Studi di Firenze, I-50121, Firenze, Italy E-mail: [email protected] Received 19 May 2010, in final form 22 June 2010 Published 21 September 2010 Online at stacks.iop.org/CQG/27/194002 Abstract Advanced gravitational wave interferometers, currently under realization, will soon permit the detection of gravitational waves from astronomical sources. To open the era of precision gravitational wave astronomy, a further substantial improvement in sensitivity is required. The future space-based Laser Interferometer Space Antenna and the third-generation ground-based observatory Einstein Telescope (ET) promise to achieve the required sensitivity improvements in frequency ranges. The vastly improved sensitivity of the third generation of gravitational wave observatories could permit detailed measurements of the sources’ physical parameters and could complement, in a multi-messenger approach, the observation of signals emitted by cosmological sources obtained through other kinds of telescopes. This paper describes the progress of the ET project which is currently in its design study phase. 2 Class. Quantum Grav. 27 (2010) 194002 M Punturo et al PACS number: 40.80.Nn (Some figures in this article are in colour only in the electronic version) 1. Introduction Interferometric gravitational wave (GW) detectors have demonstrated the validity of their working principle by coming close to, or even exceeding, the design sensitivity of the initial instruments: LIGO [1], Virgo [2], GEO600 [3] and TAMA [4]. In the same infrastructures, currently hosting the initial GW detectors (and their limited upgrades, called ‘enhanced’ interferometers: eLIGO and Virgo+) a second generation of interferometers (so-called advanced detectors: ‘Advanced LIGO’ [5], ‘Advanced Virgo’ [6] and GEO-HF [3]) will be implemented over the next few years. The Laser Interferometer Space Antenna (LISA), a joint ESA–NASA mission expected to fly around 2020, is a space-borne detector to observe in the frequency range of 0.1 mHz–0.1 Hz—a frequency range that is not accessible from ground. These detectors, based on technologies currently available, and partly already tested in reduced-scale prototypes, but still to be implemented in full scale, will show a sensitivity improved roughly by a factor of 10 with respect to the initial interferometers. Hence, a detection rate about a factor of 1000 larger than with the initial interferometers is expected, strongly enhancing the probability of detecting the signals generated by astro-physical sources. In particular, considering the predicted detection rate of the GW signal generated by a binary system of coalescing neutron stars [7], the sensitivity of the advanced interferometers is expected to guarantee the detection within months to a year at most. Apart from extremely rare events, the signal-to-noise ratio (SNR) of detections in the ‘advanced’ detectors is likely to be still too low for precise astronomical studies of the GW sources and for complementing optical and x-ray observations in the study of fundamental systems and processes in the Universe. This consideration led the GW community to investigate the possibility of building a new (third) generation of detectors, permitting both to observe, with huge SNR, GW sources at distances similar to those detectable in the advanced detectors and to reveal GW signals at distances comparable with the sight distance of 6 electromagnetic telescopes. As LISA will do for super-massive black holes (M 10 MSun), the Einstein Telescope (ET), thanks to this capability to inspect the GW signal in great detail, could herald a new era of routine GW astronomy for lighter astrophysical bodies. To realize a third-generation GW observatory, with a significantly enhanced sensitivity (considering a target of a factor of 10 improvement over advanced detectors in a wide frequency range), several limitations of the technologies adopted in the advanced interferometers must be overcome and new solutions must be developed to reduce the fundamental and technical noises that will limit the next-generation detectors. But, mainly, new research facilities hosting the third-generation GW observatory apparatuses must be realized, to circumvent the limitations imposed by the current facilities. Hereafter, we will describe some of the possible scientific goals and some of the challenges of a third-generation GW observatory, as evaluated within the framework of the ET design study [8].
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